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Properties and Occurrence Rates for Kepler Exoplanet Candidates as a Function of Host Star Metallicity from the DR25 Catalog

Narang, Mayank and Manoj, P. and Furlan, E. and Mordasini, C. and Henning, Thomas and Mathew, Blesson and Banyal, Ravinder K. and Sivarani, T. (2018) Properties and Occurrence Rates for Kepler Exoplanet Candidates as a Function of Host Star Metallicity from the DR25 Catalog. Astronomical Journal, 156 (5). Art. No. 221. ISSN 1538-3881. https://resolver.caltech.edu/CaltechAUTHORS:20181025-110845725

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Abstract

Correlations between the occurrence rate of exoplanets and their host star properties provide important clues about the planet formation process. We studied the dependence of the observed properties of exoplanets (radius, mass, and orbital period) as a function of their host star metallicity. We analyzed the planetary radii and orbital periods of over 2800 Kepler candidates from the latest Kepler data release, DR25 (Q1–Q17), with revised planetary radii based on Gaia DR2 as a function of host star metallicity (from the Q1–Q17 (DR25) stellar and planet catalog). With a much larger sample and improved radius measurements, we are able to reconfirm previous results in the literature. We show that the average metallicity of the host star increases as the radius of the planet increases. We demonstrate this by first calculating the average host star metallicity for different radius bins and then supplementing these results by calculating the occurrence rate as a function of planetary radius and host star metallicity. We find a similar trend between host star metallicity and planet mass: the average host star metallicity increases with increasing planet mass. This trend, however, reverses for masses >4.0 M_J: host star metallicity drops with increasing planetary mass. We further examined the correlation between the host star metallicity and the orbital period of the planet. We find that for planets with orbital periods less than 10 days, the average metallicity of the host star is higher than that for planets with periods greater than 10 days.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-3881/aae391DOIArticle
https://arxiv.org/abs/1809.08385arXivDiscussion Paper
ORCID:
AuthorORCID
Manoj, P.0000-0002-3530-304X
Furlan, E.0000-0001-9800-6248
Mordasini, C.0000-0002-1013-2811
Mathew, Blesson0000-0002-7254-191X
Additional Information:© 2018 The American Astronomical Society. Received 2018 June 21; revised 2018 September 20; accepted 2018 September 20; published 2018 October 25. We thank the referee for insightful comments and suggestions that have led to the improvement of the final manuscript. CM acknowledges support from the Swiss National Science Foundation under grant BSSGI0_155816, "PlanetsInTime." Parts of this work have been carried out within the frame of the National Center for Competence in Research PlanetS, supported by the SNSF. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This research has also made use of NASA's Astrophysics Data System Abstract Service and the SIMBAD database, operated at CDS, Strasbourg, France.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
Swiss National Science Foundation (SNSF)BSSGI0_155816
Subject Keywords:methods: statistical – planets and satellites: formation – planets and satellites: general – stars: abundances – stars: fundamental parameters
Issue or Number:5
Record Number:CaltechAUTHORS:20181025-110845725
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20181025-110845725
Official Citation:Mayank Narang et al 2018 AJ 156 221
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:90415
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:25 Oct 2018 18:13
Last Modified:07 Nov 2019 00:16

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